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& \\
\multicolumn{1}{|l|}{\hspace{0.5cm}\LARGE\bf\sf Active}
& \multicolumn{1}{|c|}{\large\em An electronic publication dedicated to}\\ [0.3cm]
\multicolumn{1}{|l|}{\hspace{0.5cm}\LARGE\bf\sf Galaxies} & \multicolumn{1}{|c|}{\large\em the observation and theory of}\\ [0.3cm]
\multicolumn{1}{|l|}{\hspace{0.5cm}\LARGE\bf\sf Newsletter} & \multicolumn{1}{|c|}{\large\em active galaxies}\\ [0.3cm]
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& \\
\multicolumn{1}{|c|}{\large\bf\sf No. 38 --- May 2000 } &
\multicolumn{1}{|c|}{\bf\sf Editor: Matt Redman (mpr@ast.man.ac.uk)} \\ [-0.1cm]
& \\ \hline
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\small
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{\Large\em Abstracts - Thesis Abstracts - Jobs - Meetings}
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{\Large\sf From the Editor}
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\vspace*{0.6cm}
The Active Galaxies Newsletter is produced monthly. The deadline for
contributions is the last friday of the month. The Latex macros for
submitting abstracts and dissertation abstracts are appended to each
issue of the newsletter and are also available on the web page.
\newline Matt Redman
\vspace*{1cm}
\begin{center}
{\Large\sf Abstracts of recently accepted papers}
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\vspace*{0.6cm}
{\large\bf{Double-Peaked Broad Emission Lines in NGC 4450 and Other LINERs}}
{\bf{ Luis C. Ho$^{1,2}$, Greg Rudnick$^2$, Hans-Walter Rix$^3$, Joseph C.
Shields$^4$, Daniel H. McIntosh$^2$, Alexei V. Filippenko$^5$,
Wallace L. W. Sargent$^6$, and Michael Eracleous$^7$}}
$^1$ {Carnegie Observatories, 813 Santa Barbara St., Pasadena, CA
91101-1292}\\
$^2$ {Steward Observatory, Univ. of Arizona, Tucson, AZ
85721.}\\
$^3$ {Max-Planck-Institut f\"{u}r Astronomie, K\"{o}nigstuhl 17, Heidelberg,
D-69117, Germany.}\\
$^4$ {Ohio University, Dept. of Physics and Astronomy, Clippinger Labs 251B,
Athens, OH 45701-2979.}\\
$^5$ {Department of Astronomy, University of California, Berkeley,
CA 94720-3411.}\\
$^6$ {Palomar Observatory, 105-24 Caltech, Pasadena, CA 91125.}\\
$^7$ {Department of Astronomy and Astrophysics, The Pennsylvania State,
University, 525 Davey Lab, University Park, PA 16802.}
\def\hst{{\it HST}}
{Spectra taken with the {\it Hubble Space Telescope} (\hst) reveal
that NGC 4450 emits Balmer emission lines with displaced double peaks
and extremely high-velocity wings. This characteristic line profile,
previously seen in a few nearby LINERs and in a small fraction of
broad-line radio galaxies, can be interpreted as a kinematic signature
of a relativistic accretion disk. We can reproduce the observed
profile with a model for a disk with a radial range of 1000--2000
gravitational radii and inclined by 27 degrees along the line of
sight. The small-aperture \hst\ data also allow us to detect, for the
first time, the featureless continuum at optical wavelengths in NGC
4450; the nonstellar nucleus is intrinsically very faint, with $M_B$ =
--11.2 mag for $D$ = 16.8 Mpc.
We have examined the multiwavelength properties of NGC 4450
collectively with those of other low-luminosity active nuclei which
possess double-peaked broad lines and find a number of common
features. These objects are all classified spectroscopically as
``type 1'' LINERs or closely related objects. The nuclear
luminosities are low, both in absolute terms and relative to the
Eddington rates. All of them have compact radio cores, whose strength
relative to the optical nuclear emission places them in the league of
radio-loud active nuclei. The broad-band spectral energy
distributions of these sources are most notable for their deficit of
ultraviolet emission compared to those observed in luminous Seyfert~1
nuclei and quasars. The double-peaked broad-line radio galaxies Arp
102B and Pictor~A have very similar attributes. We discuss how these
characteristics can be understood in the context of
advection-dominated accretion onto massive black holes.}
{To appear in {\it The Astrophysical Journal.}}
{E-mail contact: lho@ociw.edu; \newline preprint available at
http://www.ociw.edu/$\sim$lho/}
\vspace*{0.6cm}
{\large\bf{Evidence for a Black Hole and Accretion Disk in the LINER NGC 4203}}
{\bf{ Joseph C. Shields$^1$, Hans-Walter Rix$^2$, Daniel H. McIntosh$^3$,
Luis C. Ho$^{3,4}$, Greg Rudnick$^3$, Alexei V. Filippenko$^5$, Wallace L. W.
Sargent$^6$, and Marc Sarzi$^{2,7}$}}
$^1$ {Ohio University, Dept. of Physics and Astronomy, Clippinger Labs 251B,
Athens, OH 45701-2979.}\\
$^2$ {Max-Planck-Institut f\"{u}r Astronomie, K\"{o}nigstuhl 17,
Heidelberg, D-69117, Germany.}\\
$^3$ {Steward Observatory, Univ. of Arizona, Tucson, AZ 85721.}\\
$^4$ {Carnegie Observatories, 813 Santa Barbara St., Pasadena, CA 91101-1292,
Steward Observatory, Univ. of Arizona, Tucson, AZ 85721.}\\
$^5$ {Department of Astronomy, University of California, Berkeley,
CA 94720-3411.}\\
$^6$ {Palomar Observatory, 105-24 Caltech, Pasadena, CA 91125.}\\
$^7$ {Dipartimento di Astronomina, Universit\'a di Padova,
vicolo dell'Osservatorio 5 I-35122, Italy.}
{We present spectroscopic observations from the Hubble Space Telescope that
reveal for the first time the presence of a broad pedestal of Balmer-line
emission in the LINER galaxy NGC 4203. The emission-line profile is suggestive
of a relativistic accretion disk, and is reminiscent of double-peaked
transient Balmer emission observed in a handful of other LINERs. The very
broad line emission thus constitutes clear qualitative evidence for a black
hole, and spatially resolved narrow-line emission in NGC 4203 can be used to
constrain its mass, with $M_{\rm BH}\,}{_{\sim}}\else$\stackrel{>}{_{\sim}}$\fi}
\begin{center}
{\Large\bf{Molecular Gas in Seyfert Galaxies}}
\vspace*{0.5cm}
{\bf{S. J. Curran}}
{Thesis work conducted at: Onsala Space Observatory with the
Department of Radio and Space Science, Chalmers University of
Technology, G\"{o}teborg, Sweden}
{Current address: European Southern Observatory, Casilla 19001,
Santiago 19, Chile}
{Electronic mail: scurran@eso.org}
{Ph.D dissertation directed by: Roy Booth and Lars E. B. Johansson}
{Ph.D degree awarded: March 2000}
\vspace*{0.8cm}
\end{center}
{In this report we present the results of a single dish study of the
molecular gas properties in Seyfert galaxies. From the observations of
the closest lying example, the Circinus galaxy, we find that about
half of the molecular gas is distributed in a circumnuclear ring
orbiting the central super-massive black hole, believed to be powering
this type 2 Seyfert. The 100 pc-scale ring orbits with non-Keplerian
rotation at a maximum velocity of $\approx180$~\hbox{${\rm km\
s}^{-1}$.} From this we deduce that the $N_{{\rm H}_{2}}/I_{{\rm CO}}$
Galactic conversion ratio causes us to overestimate the gas mass
fraction by a factor of $\approx5$. From further studies, the
remainder of the gas appears to be in a 90$^{\circ}$ ~wide outflow
which extends to $\pm500$~pc along the rotation axis of the ring. The
maximum outflow velocity of $\approx\pm190$~\hbox{${\rm km\ s}^{-1}$}
~gives a mechanical luminosity of $\gapp10^7$L$_\odot$ ~and the
orientation of the outflow axis suggests that the molecular ring is
very nearly coplanar with the central body obscuring the active
galactic nucleus.
By observing a sample of 20 Seyfert galaxies, we find that the HCN to
CO luminosity ratio, $\frac{L_{\rm HCN}}{L_{\rm CO}}\approx1/6$, is
considerably higher than for normal spiral galaxies and comparable to
the ratios found in ultra-luminous infra-red galaxies (ULIRGs). Our
observations suggest that there may be differences in the molecular
gas distributions between low ($L_{\rm FIR}\sim10^{10}~{\rm
L}_{\odot}$) and high ($L_{\rm FIR}\sim10^{11}~{\rm L}_{\odot}$) far
infra-red luminous (FIR) Seyferts. By combining our results with the
FIR luminosities, we find that $\frac{L_{\rm FIR}}{L_{\rm CO}}~(L_{\rm
FIR}\sim10^{11}~{\rm L}_{\odot}~{\rm Seyferts})\approx10\frac{L_{\rm
FIR}}{L_{\rm CO}}~({\rm normal ~spirals})$ and $\frac{L_{\rm
FIR}}{L_{\rm HCN}}~({\rm Seyferts})\approx\frac{L_{\rm FIR}}{L_{\rm
HCN}}~({\rm ULIRGs})\approx\frac{L_{\rm FIR}}{L_{\rm HCN}}~({\rm
normal ~spirals})$. From this we cannot ascertain the relative
radiation contribution of the star-burst and the active nucleus,
although between NGC 4945 and Circinus, in which we have performed
multi-transitional observations, these seem to differ. This may have
the effect of lowering current estimates of the star formation rates
in Seyfert galaxies, although both galaxies do appear to have
relatively high populations ({\rm c.f.} the Galaxy) of massive
($\gapp10{\rm M}_{\odot}$) stars. Finally, estimates of the gas
inclinations in these 20 Seyferts appear to suggest that the various
gas disk structures on all scales are usually aligned in each galaxy,
supporting the notion that the obscuration may be but a dense
component of the large-scale gas structure. }
\newpage
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{\Large\sf Meetings}
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{\large\bf{QSO hosts and their environments}}\\ Granada, Spain\\ 10-12
January 2001
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This 3 days workshop will be devoted to the revision of the {\it state
of the art} on QSO hosts and their environments,
the multi-wavelength properties of these
objects till look back times, and their implications in galaxy formation
and
evolution.
The main topics to be summarized will be the following:
- Hosts of radio-loud and radio-quiet QSOs and their redshift evolution.
Black hole formation, growth, relation to host galaxy, and fuelling.
- BL-Lacs and radio galaxies as related phenomena in unification
framework.
- QSO luminosity, the effect of beaming and dust.
Evolution of AGN luminosity function and energy balance in the Universe.
High redshift QSOs as tracers of structures and galaxy formation.
- Effects of tidal interacions/mergers.
- Cluster environment and its redshift evolution.
Scientific Organising Comitee:
John N. Bahcall, Institute for Advanced Study, Princeton (USA)
Malcolm Bremer \hskip 1truecm Bristol University (United Kingdom)
Deborah Dultzin-Hacyan, Instituto de Astronom\'{\i}a, UNAM (Mexique)
James Dunlop, John Moore University, Liverpool (United Kingdom)
Jochen Heidt, Landessternwarte, Heidelberg (Germany)
John Hutchings, Dominion Astroph. Observatory, Victoria (Canada)
Isabel M\'arquez, IAA (CSIC), Granada (Spain)
Patrick Petitjean, IAP, Paris (France)
The first announcement of this workshop will be available in May 2000.
We are limited to a maximum of 60 people.
FOR FURTHER INFORMATION PLEASE CONTACT THE CONFERENCE ORGANISER:
Isabel Marquez, E-mail: isabel@iaa.es, FAX: +34 958 81 45 30
Meeting home page: http://www.iaa.csic.es/$\sim$qsoenv/
\newpage
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{\Large\sf Announcements}
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{\large\bf{The Tartarus Database of ASCA Observations of AGN:\\
Version 2 - May 5 2000 }}
\end{center}
\vspace*{0.6cm}
{\bf{ T.J.Turner$^{1,2}$ \& K.Nandra$^{2,3}$ }}
$^1$ { University of Maryland Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA } \\
$^2$ {Laboratory for High Energy Astrophysics, Code 662, NASA/GSFC, Greenbelt, MD 20771, USA } \\
$^3$ {Universities Space Research Association, Greenbelt MD, USA}
{We are happy to announce the release of version 2 of the Tartarus
database. This version of the database contains 529 reduced sequences,
and includes everything in the public archives up to May 3 2000. The
main improvement over version 1 is a refinement of the source
detection routine so that, even when the target AGN is very faint, it
will be extracted correctly, even in the presence of a bright
serendipitous source.
For more details, please visit:
\verb+ http://tartarus.gsfc.nasa.gov/ +
{\bf ACCESS VIA W3BROWSE:}
Tartarus pages and products will shortly (within a few weeks)
be available via the W3BROWSE interface.
{\bf NOTE: }
Some sequences have failed the automatic processing, and some
suffer contamination of source or background regions by a
serendipitous source. Those sequences will be fixed as time
allows, and we will give highest priority to fix sequences
that have been requested. Please send requests/comments
to our helpdesk at:
\verb+ tartarus@olegacy.gsfc.nasa.gov +
If you have received this message erroneously or do not wish
to receive further updates, please reply to this e-mail and we
will remove your name from our list.
Best Regards,
The Tartarus Team
\verb+ http://tartarus.gsfc.nasa.gov/doc/team.html +
}
{ }
{E-mail contact: tartarus@olegacy.gsfc.nasa.gov}
\vspace*{0.6cm}
\begin{center}
{\large\bf{Release of the INES Archive}}
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\vspace*{0.6cm}
The International Ultraviolet Explorer (IUE) Archives have been delivered
to the world scientific community on 21st March. ESA, in collaboration with
the Spanish Laboratory of Space Astrophysics and Theoretical Physics
(LAEFF) belonging to INTA (National Institute of Air and Space Technology),
has developed and set up the INES system to access IUE Data.
INES (IUE Newly Extracted Spectra) is a complete astronomical archive and
data-distribution system. Its release to the community represents the final
activity by ESA in the context of the IUE project. From now LAEFF, on
behalf of the international astronomical community, will be responsible of
maintaining INES, making it available and providing world-wide support to
scientists using IUE data.
The IUE Archive contains more than 110,000 spectra of more that 11,000
astronomical objects. All data are fully reduced and calibrated. The INES
archive consists of:
- an access catalog containing the parameters required to query the
archive and evaluate the observations,
- a publications catalog which links each spectrum to the publications
in which it has been used via the ADS,
- and the data themselves (low dispersion spectra, high dispersion
spectra rebinned to the low resolution wavelength step, full high
dispersion concatenated spectra, and bi-dimensional low dispersion
images).
The INES Archive can be accessed at http://ines.vilspa.esa.es. Users
can consult the catalogue, preview the spectra and download the data
with a standard browser from the Principal Centre at LAEFF, its Mirror
Centre located at the Canadian Astronomical Data Centre or any of the
National Centres spread in all continents. This distributed system
guarantees the availability and efficient access to the data.
Questions about the INES archive can be directed to the INES Help Desk
at
ineshelp@iuearc.vilspa.esa.es
or at
http://iuearc.vilspa.esa.es/ines\_jb/HelpDesk/
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{
The Active Galaxies Newsletter is available on the World Wide Web.
You can access it via the University of Manchester home page :-
http://www.ast.man.ac.uk/$\sim$mpr/agn/
\vspace*{0.3cm}
If you move or your e-mail address changes, please send the editor
your new address. If the Newsletter repeatedly bounces back from an
address then that address is deleted from the mailing list.
}}}
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